Collisional Evolution of the Outer Asteroid Belt

Icarus ◽  
2000 ◽  
Vol 145 (2) ◽  
pp. 382-390 ◽  
Author(s):  
R Gil-Hutton
Keyword(s):  
Asteroid Belt ◽  
Collisional Evolution

scholarly journals New multi-part collisional model of the main belt: the contribution to near-Earth asteroids

2020 ◽  
Vol 639 ◽  
pp. A9
Author(s):  
P. S. Zain ◽  
G. C. de Elía ◽  
R. P. Di Sisto
Keyword(s):  
Significant Contribution ◽  
Asteroid Belt ◽  
Size Distributions ◽  
Main Belt ◽  
Yarkovsky Effect ◽  
Source Regions ◽  
Main Asteroid Belt ◽  
Near Earth Asteroids ◽  
Asteroid Families ◽  
Collisional Evolution

Aims. We developed a six-part collisional evolution model of the main asteroid belt (MB) and used it to study the contribution of the different regions of the MB to the near-Earth asteroids (NEAs). Methods. We built a statistical code called ACDC that simulates the collisional evolution of the MB split into six regions (namely Inner, Middle, Pristine, Outer, Cybele and High-Inclination belts) according to the positions of the major resonances present there (ν6, 3:1J, 5:2J, 7:3J and 2:1J). We consider the Yarkovsky effect and the mentioned resonances as the main mechanism that removes asteroids from the different regions of the MB and delivers them to the NEA region. We calculated the evolution of the NEAs coming from the different source regions by considering the bodies delivered by the resonances and mean dynamical timescales in the NEA population. Results. Our model is in agreement with the major observational constraints associated with the MB, such as the size distributions of the different regions of the MB and the number of large asteroid families. It is also able to reproduce the observed NEAs with H < 16 and agrees with recent estimations for H < 20, but deviates for smaller sizes. We find that most sources make a significant contribution to the NEAs; however the Inner and Middle belts stand out as the most important source of NEAs followed by the Outer belt. The contributions of the Pristine and Cybele regions are minor. The High-Inclination belt is the source of only a fraction of the actual observed NEAs with high inclination, as there are dynamical processes in that region that enable asteroids to increase and decrease their inclinations.

The Collisional Evolution of the Main Asteroid Belt

Asteroids IV ◽  
2015 ◽  
Author(s):  
W. F. Bottke ◽  
M. Brož ◽  
D. P. O’Brien ◽  
A. Campo Bagatin ◽  
A. Morbidelli ◽  
...  
Keyword(s):  
Asteroid Belt ◽  
Main Asteroid Belt ◽  
Collisional Evolution

The Collisional Evolution of the Asteroid Belt and Its Contribution to the Zodiacal Cloud

Icarus ◽  
1997 ◽  
Vol 130 (1) ◽  
pp. 140-164 ◽  
Author(s):  
Daniel D. Durda ◽  
Stanley F. Dermott
Keyword(s):  
Asteroid Belt ◽  
Zodiacal Cloud ◽  
Collisional Evolution

Collisional evolution of the early asteroid belt

1999 ◽  
Vol 47 (3-4) ◽  
pp. 331-338 ◽  
Author(s):  
Ricardo Gil-Hutton ◽  
Adrián Brunini
Keyword(s):  
Asteroid Belt ◽  
Collisional Evolution

scholarly journals Very early collisional evolution in the asteroid belt

2001 ◽  
Vol 53 (11) ◽  
pp. 1093-1097 ◽  
Author(s):  
Stuart J Weidenschilling ◽  
Donald R Davis ◽  
Francesco Marzari
Keyword(s):  
Asteroid Belt ◽  
Collisional Evolution

Collisional evolution of the asteroid belt

Icarus ◽  
2004 ◽  
Vol 169 (2) ◽  
pp. 357-372 ◽  
Author(s):  
Andrew F Cheng
Keyword(s):  
Asteroid Belt ◽  
Collisional Evolution

Collisional reaccumulation of asteroids

1999 ◽  
Vol 173 ◽  
pp. 145-152
Author(s):  
A. Campo Bagatin ◽  
P. Farinella
Keyword(s):  
Size Distribution ◽  
Size Range ◽  
Asteroid Belt ◽  
Evolution Process ◽  
Diameter Range ◽  
Main Asteroid Belt ◽  
Collisional Evolution

AbstractWe have developed a new version of the code developed by Campo Bagatin (1994a, b) to model the collisional evolution of the asteroid size distribution. The new code distinguishes between “intact”, unfractured asteroids and asteroids converted by energetic collisions into “piles of rubble”. We have run a number of simulations of the collisional evolution process to assess the size range where reaccumulated bodies should be expected to be abundant in the main asteroid belt. We find that this diameter range ranges from about 10 to 100 km, but may extend to smaller or larger bodies depending on the prevailing collisional response parameters.

Comments on collision mechanics in ring systems

1984 ◽  
Vol 75 ◽  
pp. 407-422
Author(s):  
William K. Hartmann
Keyword(s):  
Asteroid Belt ◽  
Surface Erosion ◽  
Surface Layers ◽  
Ring Systems ◽  
Eclipse Observations ◽  
Saturn’S Rings ◽  
Saturn's Rings

ABSTRACTThe nature of collisions within ring systems is reviewed with emphasis on Saturn's rings. The particles may have coherent icy cores and less coherent granular or frosty surface layers, consistent with thermal eclipse observations. Present-day collisions of such ring particles do not cause catastrophic fragmentation of the particles, although some minor surface erosion and reaccretion is possible. Evolution by collisional fragmentation is thus not as important as in the asteroid belt.

scholarly journals Organic matter and water from asteroid Itokawa

2021 ◽  
Vol 11 (1) ◽  
Author(s):  
Q. H. S. Chan ◽  
A. Stephant ◽  
I. A. Franchi ◽  
X. Zhao ◽  
R. Brunetto ◽  
...  
Keyword(s):  
Organic Matter ◽  
Solar System ◽  
Parent Body ◽  
Asteroid Belt ◽  
True Nature ◽  
Water Ice ◽  
Nanocrystalline Graphite ◽  
Terrestrial Water ◽  
Solar System Bodies ◽  
Small Dust

AbstractUnderstanding the true nature of extra-terrestrial water and organic matter that were present at the birth of our solar system, and their subsequent evolution, necessitates the study of pristine astromaterials. In this study, we have studied both the water and organic contents from a dust particle recovered from the surface of near-Earth asteroid 25143 Itokawa by the Hayabusa mission, which was the first mission that brought pristine asteroidal materials to Earth’s astromaterial collection. The organic matter is presented as both nanocrystalline graphite and disordered polyaromatic carbon with high D/H and 15N/14N ratios (δD =  + 4868 ± 2288‰; δ15N =  + 344 ± 20‰) signifying an explicit extra-terrestrial origin. The contrasting organic feature (graphitic and disordered) substantiates the rubble-pile asteroid model of Itokawa, and offers support for material mixing in the asteroid belt that occurred in scales from small dust infall to catastrophic impacts of large asteroidal parent bodies. Our analysis of Itokawa water indicates that the asteroid has incorporated D-poor water ice at the abundance on par with inner solar system bodies. The asteroid was metamorphosed and dehydrated on the formerly large asteroid, and was subsequently evolved via late-stage hydration, modified by D-enriched exogenous organics and water derived from a carbonaceous parent body.

scholarly journals A thermophysical and dynamical study of the Hildas (1162) Larissa and (1911) Schubart

2021 ◽  
Author(s):  
Cristian F Chavez ◽  
T G Müller ◽  
J P Marshall ◽  
J Horner ◽  
H Drass ◽  
...  
Keyword(s):  
Thermal Inertia ◽  
Infrared Camera ◽  
Asteroid Belt ◽  
Effective Diameter ◽  
Early Solar System ◽  
Dynamical Study ◽  
Axis Ratio ◽  
Ellipsoidal Shape ◽  
Dynamical Simulations ◽  
Taxonomical Classification

Abstract The Hilda asteroids are among the least studied populations in the asteroid belt, despite their potential importance as markers of Jupiter’s migration in the early Solar system. We present new mid-infrared observations of two notable Hildas, (1162) Larissa and (1911) Schubart, obtained using the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST), and use these to characterise their thermal inertia and physical properties. For (1162) Larissa, we obtain an effective diameter of 46.5$^{+2.3}_{-1.7}$ km, an albedo of 0.12 ± 0.02, and a thermal inertia of 15$^{+10}_{-8}$ Jm−2s1/2K−1. In addition, our Larissa thermal measurements are well matched with an ellipsoidal shape with an axis ratio a/b=1.2 for the most-likely spin properties. Our modelling of (1911) Schubart is not as refined, but the thermal data point towards a high-obliquity spin-pole, with a best-fit a/b=1.3 ellipsoidal shape. This spin-shape solution is yielding a diameter of 72$^{+3}_{-4}$ km, an albedo of 0.039± 0.02, and a thermal inertia below 30 Jm−2s1/2K−1 (or 10$^{+20}_{-5}$ Jm−2s1/2K−1). As with (1162) Larissa, our results suggest that (1911) Schubart is aspherical, and likely elongated in shape. Detailed dynamical simulations of the two Hildas reveal that both exhibit strong dynamical stability, behaviour that suggests that they are primordial, rather than captured objects. The differences in their albedos, along with their divergent taxonomical classification, suggests that despite their common origin, the two have experienced markedly different histories.

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